Away from the reconnection region, in slit position 4 at 02:05:36 UT, we compute the line integrated intensities by fitting the observed profiles with Gaussian functions
using the xcfit.pro fitting routine.
Typically, two Gaussian functions were needed to fit each line profile of Si IV, in the mini-flare area
between y = 76 and 88. The two Gaussian functions
are separated by up to \(\approx \) 0.4 Å, one function has a narrow Full Width half maximum (FWHM) and the other one an extended FWHM but with a lower intensity [1]}. The two Si IV line profiles showed
similar asymmetries.
Particularly exceptional profiles of both lines were observed at y \(\approx \) 80, where the `bumps' in line red wings were considerably weaker. Based on this, we suggest that the bumps present in the profiles do not originate in blends, but in the motion of the emitting plasma. To check this assumption, we calculated synthetic spectra using CHIANTI v7.1 ([2]}; [3]}) for log(\(N_{\text{e}}\)  [cm\(^{-3}\) ]) = 11, flare DEM. Even though we found several lines blending both lines of Si IV, their contributions were found to be negligible.
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